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Black hole-neutron star (BHNS) binary mergers are candidate engines forgenerating both short-hard gamma-ray bursts (SGRBs) and detectablegravitational waves. Using our most recent conformal thin-sandwich BHNS initialdata and our fully general relativistic hydrodynamics code, which is nowAMR-capable, we are able to efficiently and accurately simulate these binariesfrom large separations through inspiral, merger, and ringdown. We evolve themetric using the BSSN formulation with the standard moving puncture gaugeconditions and handle the hydrodynamics with a high-resolution shock-capturingscheme. We explore the effects of BH spin (aligned and anti-aligned with theorbital angular momentum) by evolving three sets of initial data with BH:NSmass ratio q=3: the data sets are nearly identical, except the BH spin isvaried between a/M = -0.5 (anti-aligned), 0.0, and 0.75. The number of orbitsbefore merger increases with a/M, as expected. We also study the nonspinning BHcase in more detail, varying q between 1, 3, and 5. We calculate gravitationalwaveforms for the cases we simulate and compare them to binary black-holewaveforms. Only a small disk (< 0.01 M_sun) forms for the anti-aligned spincase (a/M = -0.5) and for the most extreme mass ratio case (q=5). By contrast,a massive (M_disk is about 0.2 M_sun), hot disk forms in the rapidly spinning(a/M = 0.75) aligned BH case. Such a disk could drive a SGRB,possibly by, e.g.,producing a copious flux of neutrino-antineutino pairs.

Relativistic Simulations of Black Hole-Neutron Star Mergers: Effects of black-hole spin